학술논문
CEERS: Spatially Resolved UV and mid-IR Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes
Document Type
Working Paper
Author
Shen, Lu; Papovich, Casey; Yang, Guang; Matharu, Jasleen; Wang, Xin; Magnelli, Benjamin; Elbaz, David; Jogee, Shardha; Alavi, Anahita; Haro, Pablo Arrabal; Backhaus, Bren E.; Bagley, Micaela B.; Bell, Eric F.; Bisigello, Laura; Calabrò, Antonello; Cooper, M. C.; Costantin, Luca; Daddi, Emanuele; Dickinson, Mark; Finkelstein, Steven L.; Fujimoto, Seiji; Giavalisco, Mauro; Grogin, Norman A.; Guo, Yuchen; Holwerda, Benne W.; Kartaltepe, Jeyhan S.; Koekemoer, Anton M.; Kurczynski, Peter; Lucas, Ray A.; Peŕez-Gonzaĺez, Pablo G.; Pirzkal, Nor; Prichard, Laura; Rafelski, Marc; Ronayne, Kaila; Simons, Raymond C.; Sunnquist, Ben; Teplitz, Harry I.; Trump, Jonathan R.; Weiner, Benjamin J.; Windhorst, Rogier A.; Yung, L. Y. Aaron
Source
Subject
Language
Abstract
We present the mid-IR (MIR) morphologies for 64 star-forming galaxies at $0.210^{9}~M_\odot}$ using JWST MIRI observations from the Cosmic Evolution Early Release Science survey (CEERS). The MIRI bands span the MIR (7.7--21~$\mu$m), enabling us to measure the effective radii ($R_{\rm{eff}}$) and S\'{e}rsic indexes of these SFGs at rest-frame 6.2 and 7.7 $\mu$m, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We define a ``PAH-band'' as the MIRI bandpass that contains these features at the redshift of the galaxy. We then compare the galaxy morphologies in the PAH-bands to those in rest-frame Near-UV (NUV) using HST ACS/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS, where the NUV-band and F160W trace the profile of (unobscured) massive stars and the stellar continuum, respectively. The $R_{\rm{eff}}$ of galaxies in the PAH-band are slightly smaller ($\sim$10\%) than those in F160W for galaxies with $\rm{M_*\gtrsim10^{9.5}~M_\odot}$ at $z\leq1.2$, but the PAH-band and F160W have a similar fractions of light within 1 kpc. In contrast, the $R_{\rm{eff}}$ of galaxies in the NUV-band are larger, with lower fractions of light within 1 kpc compared to F160W for galaxies at $z\leq1.2$. Using the MIRI data to estimate the $\rm{SFR_{\rm{IR}}}$ surface density, we find the correlation between the $\rm{SFR_{\rm{IR}}}$ surface density and stellar mass has a steeper slope than that of the $\rm{SFR_{\rm{UV}}}$ surface density and stellar mass, suggesting more massive galaxies having increasing amounts of obscured fraction of star formation in their inner regions. This paper demonstrates how the high-angular resolution data from JWST/MIRI can reveal new information about the morphology of obscured-star formation.
Comment: 28 pages, 11 figures, Accepted by ApJ
Comment: 28 pages, 11 figures, Accepted by ApJ